The Moons of the Planets

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C – The Planets Exercise C4: The Moons of the Planets Student name: ________________________ Class: ____________ Date: _____________ Check the box with the correct answer. Question 1: What factor, more than any other, do you think led to Jupiter having so many moons compared to the inner terrestrial planets? a. The Sun is far enough away from Jupiter that its heat is insufficient to melt icy particles orbiting the planet; these particles coalesced to form moons. b. Jupiter's rapid rotation was important in spinning off most of these moons from its surface. c. Jupiter has an extensive atmosphere from which these moons have been formed. d. The powerful gravitational field produced by Jupiter's large mass has allowed this planet to capture moons from the nearby asteroid belt. Question 2: The Galilean satellites, in order of decreasing diameter, are: a. Ganymede, Callisto, Io, Europa b. Ganymede, Io, Callisto, Europa c. Europa, Io, Callisto, Ganymede d. Io, Europa, Callisto, Ganymede Question 3: Mercury has a diameter of 4,800 km. Which of the Galilean moons of Jupiter is larger than Mercury? a. Io b. Europa c. Callisto d. Ganymede Starry Night College Version 7 1 Question 4: Which factor or factors, more than any other, have allowed Titan to retain an atmosphere? a. Its many active volcanoes continuously replenish the atmosphere with gas, which is continuously escaping into space. b. The molecular constituents of its atmosphere are heavy and cannot therefore escape Titan's gravity c. Its surface temperature is too low to allow the nitrogen gas in its atmosphere to escape from Titan's gravitational force. d. Its gravitational force has allowed it to acquire atmospheric gases from Saturn. Question 5: Phobos and Deimos most closely resemble: a. Asteroids b. Comets c. Planets d. Dwarf planets Starry Night College Version 7 2 .

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Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur To cite this version: Alex Soumbatov-Gur. Phobos, Deimos: Formation and Evolution. [Research Report] Karpov institute of physical chemistry. 2019. hal-02147461 HAL Id: hal-02147461 https://hal.archives-ouvertes.fr/hal-02147461 Submitted on 4 Jun 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur The moons are confirmed to be ejected parts of Mars’ crust. After explosive throwing out as cone-like rocks they plastically evolved with density decays and materials transformations. Their expansion evolutions were accompanied by global ruptures and small scale rock ejections with concurrent crater formations. The scenario reconciles orbital and physical parameters of the moons. It coherently explains dozens of their properties including spectra, appearances, size differences, crater locations, fracture symmetries, orbits, evolution trends, geologic activity, Phobos’ grooves, mechanism of their origin, etc. The ejective approach is also discussed in the context of observational data on near-Earth asteroids, main belt asteroids Steins, Vesta, and Mars. The approach incorporates known fission mechanism of formation of miniature asteroids, logically accounts for its outliers, and naturally explains formations of small celestial bodies of various sizes.
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Mars, Phobos, and Deimos Sample Return Enabled by ARRM Alternative Trade Study Spacecraft
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Deimos and Phobos As Destinations for Human Exploration
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